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If it is not Dark it does not MatterPhotons as signature for dark matter and dark energy:
The Cast experiment at CERNon behalf of the CAST collaboration at CERN:
Dieter HH Hoffmann, Technische Universität Darmstadt
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June 17th, 2014h @ Photno Science Conference, Novosibirsk, Russia
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CERN Axion Solar Telescope
Designed by Sebastian Baum Summer Student 2014
12 years of operation and continuous renewal aiming to search for dark matter and dark energy
3S. Neff @SPSC Oct. 2014
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(1) Germany, FreiburgAlbert-Ludwigs-Universität Freiburg Horst FISCHER, Juergen FRANZ , Fritz Hertbert HEINSIUS, Donghwa KANG, Kay KÖNIGSMANN
(2) Germany, FrankfurtApplied PhysicsVladimir ARSOV, Joachim JACOBY
(3) Germany, Garching Max-Planck-Gesellschaft (MPG), Max-Planck-Institut für Extraterrestrische Physik Heinrich BRAUNINGER, Jakob ENGLHAUSER
(4) Germany, München Max-Planck-Institut für Physik, Werner-Heisenberg-Institut Rainer KOTTHAUS, Markus KUSTER, Gerhard LUTZ, Georg RAFFELT
(5) Germany, Darmstadt Technische Universitat Darmstadt, Institut für Kernphysik Theopisti DAFNI , Dieter HOFFMANN, Manfred MUTTERER, Thomas PAPAEVANGELOU, Hans RIEGE, Yannis SEMERTZIDIS
(6) Switzerland, GeneveEuropean Organization for Nuclear Research (CERN) Klaus BARTH, Martyn DAVENPORT, Rui DE OLIVEIRA, Fabio FORMENTI, Michael HASINOFF1, Igor IRASTORZA, Alfredo PLACCI, Laura STEWART, Bruno VULLIERME, Louis WALCKIERS
(7) Greece, PatrasAUniversity of PatrasSpyridon DEDOUSSIS, Christos ELEFTHERIADIS, Anastasios LIOLIOS, Argyrios NIKOLAIDIS, Ilias SAVVIDIS, Vlasios VASILEIOU, Konstantin ZIOUTAS
(8) Greece, AthensNational Center for Scientific Research "Demokritos" (NRCPS) George FANOURAKIS, Theodoros GERALIS, Katerina ZACHARIADOU
(9) Italy, PisaScuola Normale Superiore (SNS)Luigi DiLella
(10) Russia, Moskva Russian Academy of Sciences, Institute for Nuclear Research (INR) Sergei GNINENKO, Nikolai GOLOUBEV
(11) Spain, Zaragoza Universidad de Zaragoza, Facultad de Ciencias, Instituto de Física Nuclear y Altas Energías Jose CARMONA, Susana CEBRIAN, Gloria LUZON, Angel MORALES, Julio MORALES, Alfonso ORTIZ DE SOLORZANO, Marisa SARSA, Jose VILLAR
(12) United States of America, Chicago, Il University of Chicago, Enrico Fermi Institute Juan COLLAR
(13) United State of America, Columbia, Sc University of South Carolina, Department of Physics and Astronomy Frank AVIGNONE, Richard CRESWICK, Horacio FARACH
(14) France, Gif-Sur-Yvette Centre d'Etudes de Saclay (CEA-Saclay), DAPNIA Alain DELBART, Ioanis GIOMATARIS, Samuel ANDRIAMONJE
(15) Croatia, ZagrebRuder Boskovic Institute Milica KRCMAR, Ante LJUBICIC, B. LAKIC
(16) Korea, Daejon (KAIST)
Yannis Szemertzidis
Dark Matter: AXIONs, …
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Programme
o Motivation
o Axion physics
o CAST experiment
o CCD Detector and X-ray Telescope
o Data analysis - result
o Conclusions
o Outlook
Motivation
Why Axions? (since 1977)
Strong CP problem: no CP violation observed experimentally
QCD theory predicts that CP symmetry is violated in strong
interactions
CP violation ⇒ EDM of the neutron
The answer is Peccei-Quinn mechanism Introduce the ⇒ axion field a(x) interacting with the gluon field Additional Peccei-Quinn U(1) global symmetry
Particle Data Group Fermilab
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The Axion – properties
As a result a new neutral and very light particle is predicted, the Axion (Weinberg, Wilczeck)
Very weak interaction probability with matter
Couples with two photons via Primakoff Effect in any model
Spinless boson
Viable dark matter candidate (non baryonic)
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G. Raffelt
Axionsα
pseudoscalar
neutral
practically stable
phenomenology driven by the breaking scale fa and the specific axion model
Couples to photonL = g (E•B) a
Primakoff (1951) []
PRIMAKOFF EFFECT
axion-like particles
Any scalar or pseudoscalar particles:
Relic Axions – early universe
← let there be Axions
←let there be light CMB (WMAP 30-857 GHz)
←Redshift at Hubble expansion scale 68 km/s/Mps (Planck 2013)
4% - Standard Model
E.P.S. Shellard 2003
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Dark Matter Detection (Axions)
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Sunset
Photon detectors Sunrise
Photon detectors
Sunset axions
Sunrise axions
Decomissioned LHC test magnet
Rotating platform
3 X-ray detectors
X-ray Focusing Device
Decomissioned LHC test magnet
Rotating platform
3 X-ray detectors
X-ray Focusing Device
Cern Axion Solar Telescope
Expected Axion Signal•Most of the axions are emitted from the inner 20% of the Sun•Conversion probability is proportional to (BL)^2•Therefore a strong magnet ic field needs to be pointed to the sun
In CAST we expect 0.3 counts per hour from axion-photon conversion
We need low background detectors sensitive for energies from 0.3-12 keV
Solar axions – Primakoff effect
Helioscope Principle
Mean energy = 4.2 keV
Axion Luminosity =1.9 x 10-3 L◉
Axion flux = 3.8x1011 cm-2 s -1
90% of the flux
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CERN und CAST (CERN Axion Solar Telescope)
CAST
Sun tracking time-lapse / 3.5 Hours
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90 minutes of solar tracking (16° zenith) and 21 hours of background per detector per day
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Tracking System:
Calibrated and correlated to universal coordinates (GPS)
Tracking System:
Calibrated and correlated to universal coordinates (GPS)
two times a year (September&March) the sun
is within this window
two times a year (September&March) the sun
is within this window
towards sunrise
Magnet, platform, cryogenics
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Really existing experimental problems
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Tracking the Sun
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CCD-XRT Implementation at CAST
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CCD-XRT Implementation at CAST
Magnet
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CCD-XRT Implementation at CAST
Magnet
XR-Telescope
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CCD-XRT Implementation at CAST
Magnet
XR-Telescope CCD
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The X-ray Telescope Mirror System
Abrixas space mission spare telescope - 160 cm focal length 26
Wolter type 1, Grazing incidence optics
Abrixas space mission spare telescope - 160 cm focal length
Finding the focal spot
Laser spot(yearly)
X-ray finger source
(monthly)
14.5 cm2
9.4 mm2
≈ 154
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CAST phase II – principle of detection
Extending the coherence to higher axion masses...•Coherence condition (qL << 1) is recovered for a narrow mass range around mg
Ne: number of electrons/cm3
r: gas density (g/cm3)
axionsTransverse magnetic field (B)
X ray
X raydetector
L
Aaxions
Transverse magnetic field (B)Transverse magnetic field (B)X ray
X raydetector
X ray
X raydetector
X ray
X raydetector
L
A
CCD data 2009 (2009–2011)
• 114 tracking runs out of 132 (86%);• 167.5 hours of Axion sensitive exposure;• 132.47 days of background;• 0.185 counts per hour in the spot;• 8.66±0.06×10-5cts cm-2s-1keV-1 - background.
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Result – no detection ➔ exclusion plot
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Thursday 12:25 : IAXO perspectives for Solar WISP searches : I.G. Irastorza
• from catalogued data: Distance, type and position → calculated axion flux for known stars within CAST reach
Daniel Nowakowski
Daniel Nowakowski
• from catalogued data: Distance, type and position → calculated axion flux for known stars within CAST reach
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Axion solution to mysteries:
Manuel Meyer, PATRAS Workshop 2011
Strong CP Problem
TeV Transparency
Solar Corona
11 Year Solar Cycle
A. Einstein: Lens-like Action of a Star by the Deviation of light in the Gravitational Field. (Science 1936)
Note to the editor:Let me thank for your cooperation with the little publication which Mister Mandl squeezed out of me.
It is of little value, but it makes the guy happy
http://hubblesite.org/newscenter/archive/2000/07/image/c
Hoffmann, Jacoby, Zioutas
𝑣 ≈0 .2𝑐→𝑒𝑓𝑓𝑒𝑐𝑡𝑖𝑣𝑒𝑎𝑚𝑝𝑙𝑖𝑓𝑖𝑐𝑎𝑡𝑖𝑜𝑛 𝑓𝑎𝑐𝑡𝑜𝑟 𝑜𝑓 103−104
𝑡𝑎𝑛(𝛼2 )=𝐺𝑀𝑅𝑣2 , M enclosed by R; v = velocity of particle
∼0.01c c Flux enhancement up to .
Outlook
CAST is being upgraded:• New LLNL XRT optics• InGrid detector• Radiation pressure detector - Trieste
IAXO – International AXion Observatory• Signal-to-noise ratio 105 better than CAST • In approval process by CERN
No Axion signal yet, but we are working on it!
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